The origin of slow solar wind is still debated. Sources of slow solar wind could be the boundaries of coronal holes, along magnetic flux tubes expanding super-radially [1]}, [2]}, [3]}, [4]}, [5]}. The slow solar wind appears to have different components, which have been related to different properties at the very source of the wind, for example Alfvénicity, which is thought to be higher in the slow solar wind emerging from coronal holes than in the slow solar wind originating closer to the edge of streamers [6]}, [7]}, [8]}. Slow solar wind plasma could also originate from multiple reconnection processes, known as "interchange reconnection" [9]}, [10]}, [11]} occurring at the edge of streamers or pseudo-streamers [12]}, that could produce a more time-variable solar wind, along with other phenomena which are detailed in the literature (see for example section 3.2 of [13]} or[14]}).
